Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae

1. Magnetic Fields in Supernova Remnants and Pulsar-Wind Nebulae S.P. Reynolds et al. Martin, Tseng Chao Hsiung 2013/12/18

2. Which contents I will cover… • Shell Supernova Remnants: Obliquity Dependence, and Summary! • Magnetic Fields in Pulsar-Wind Nebulae. • Usually, a review paper will let you know a little, but make you feel more confused… • I hope I will not make you feel “more more” confused!

3. Shell SNR Summary • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

4. Shell SNR conclusion • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

5. Shell SNR conclusion • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

6. Shell SNR conclusion • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

7. Shell SNR conclusion • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

8. Obliquity Dependence

9. Shell SNR conclusion • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

10. Shell SNR conclusion Spectrum of GeV emission from Cas A as seen by Fermi (Abdo et al. 2010a). The solid curves are leptonic models (dots, IC; dashes, bremsstrahlung) with magnetic-field values shown. • 1. From radio observations, equipartition values of magnetic field strength are in the∼10 μG range, but there is little physical motivation to assume equipartition. • 2. Radio polarization studies show that in young SNRs, the magnetic field is largely disordered, with a small radial preponderance. In older, larger SNRs, the field is often disordered but sometimes tangential. • 3. Curvature (spectral hardening to higher frequency) is observed in the radio spectra of Tycho and Kepler. A nonlinear shock acceleration model can explain this with magnetic field strengths of 0.1–1 mG (average over the emitting regions). • 4. Thin rims of X-ray synchrotron emission in a few young remnants require B ∼50–200 μG in the rims, if they are due to synchrotron losses on down-stream-convecting electrons. However, thin radio rims are sometimes seen as well; they require that the magnetic field disappear somehow, presumably because it is a wave field which damps. • 5. Brightening and fading of small X-ray synchrotron features in G347.3-0.5 and Cas A require B ∼ 1 mG, if they represent acceleration and loss times for electrons. Fields smaller by a factor of several are possible if the fluctuations are due to strong magnetic turbulence. • 6. Large azimuthal variations in the rolloff frequency in SN 1006 and G1.9+0.3 are difficult to explain for a conventional picture of loss-limited acceleration in parallel shocks. • 7. For Cas A, the detection at GeV energies with Fermi requires B~0.1 mG to avoid overproducing the GeV emission with electron bremsstrahlung. • 8. TeV emission seen in four shell SNRs is not well explained by either leptonic or hadronic processes. However, if it is hadronic, the magnetic fields implied are of order 100 μG,whileleptonic models require much lower fields.

11. What are you talking about….

12. Magnetic Fields in PWN PWN? SNR? CRAB?

13. Definitions are always boring… Please pay a littttttttttle attention…

14. PWNe vs. SNRs • Energy Source • Radio Morphology • Radio Spectral Index • Angular Extent • Fractional Polariza- tion

15. PWNe vs. SNRs • Energy Source • SNRs result from an essentially instantaneous deposition of energy, in the form of a blast wave driven into the ISM by a supernova explosion. • PWNe have a continuous power source, the bulk relativistic flow of electron/positron pairs from an energetic neutron star.

16. PWNe vs. SNRs • Radio Morphology • SNRs are usually limb-brightened shells of synchrotron emission • PWNe are typically amorphous or filled-center synchrotron nebulae brightest at the pulsar’s position.

17. PWNe vs. SNRs • Radio Spectral Index: • SNRs usually have relatively steep radio spectral indices, α≈0.3–0.8. • PWNe have spectral indices in the range, α ≈ 0–0.3.

18. PWNe vs. SNRs • Angular Extent • SNRs are long-lived objects with a wide range of sizes, with angular extents ranging from ∼1’ to >5◦. • PWNeare usually relatively small, with sizes in therange 10’ to 30’’ , although a few older PWNe may be significantly larger.

19. PWNe vs. SNRs • Fractional Polarization • At radio frequencies near 1 GHz, SNRs typically have modest amounts of linear polarization, at the level of 5%–10%. • PWNe usually have very well organized magnetic fields, with correspondingly higher polarization fractions, in the range 30%–50%.

20. PWN Evolution the word "pwn" which is a typographical error of the word "own"

21. PWN Evolution • The expansion of the PWN • Interaction of the PWN with the surrounding SNR • The motion of the pulsar powering the PWN

22. PWN Evolution Deep Chandra image of the composite SNR G21.5-0.9 • The expansion of the PWN

23. PWN Evolution • Interaction of the PWN with the surrounding SNR 2.4 GHz Parkes image of the Vela supernova remnant. The white cross indicates the pulsar, and the arrow its proper motion .

24. PWN Evolution • The motion of the pulsar powering the PWN

25. Measuring PWN B-Fields • Various techniques • Different viewing angle • The only limited observation of B-Fields is in pulsar bow shocks

26. I think after this talk… • For PWN, maybe you know a little • For B-Field in PWN…. • If you have any question, please ask next speaker, thank you!!!